Rotation of Halo Populations in the Milky Way and M31

TL;DR

This study investigates rotational properties of various stellar populations and satellite systems in the Milky Way and M31, revealing significant rotation signals and potential common origins, with implications for galaxy formation and dark matter halo dynamics.

Contribution

Introduces simple distribution functions to model anisotropic and rotating stellar populations within dark matter halos, analyzing their kinematic properties in the Milky Way and M31.

Findings

Milky Way BHB stars show a dichotomy in rotation based on metallicity.

Milky Way globular clusters and satellites exhibit rotation with ~50 km/s.

M31's dwarf spheroidals and globular clusters show strong systemic rotation.

Abstract

We search for signs of rotation in the subsystems of the Milky Way and M31 that are defined by their satellite galaxies, their globular cluster populations, and their BHB stars. A set of simple distribution functions are introduced to describe anisotropic and rotating stellar populations embedded in dark haloes of approximate Navarro-Frenk-White form. The BHB stars in the Milky Way halo exhibit a dichotomy between a prograde rotating, comparatively metal-rich component ([Fe/H] > -2) and a retrograde rotating, comparatively metal-poor ([Fe/H] < -2) component. The prograde metal-rich population may be associated with the accretion of a massive satellite (~ 10^9 solar masses). The metal-poor population may characterise the primordial stellar halo and the net retrograde rotation could then reflect an underestimate in our adopted local standard of rest circular velocity Theta_0. If Theta_0 is ~ 240 km/s then the metal-poor component has no rotation and there is a net prograde rotation signal of ~45 km/s in the metal-rich component. There is reasonable evidence that the Milky Way globular cluster and satellite galaxy systems are rotating with <v_phi> ~50 km/s and <v_phi> ~ 40 km/s respectively. Furthermore, a stronger signal is found for the satellite galaxies when the angular momentum vector of the satellites is inclined with respect to the normal of the disc. The dwarf spheroidal satellites of M31 exhibit prograde rotation relative to the M31 disc with <v_phi> ~ 40 km/s. We postulate that this group of dwarf spheroidals may share a common origin. We also find strong evidence for systemic rotation in the globular clusters of M31 particularly for the most metal-rich.